Is there a quantum gravity effect on the cosmic microwave background power spectrum?

Is there a quantum gravity effect on the cosmic microwave background power spectrum?

Abstract

An assessment is made of recent attempts to evaluate how quantum gravity may affect the anisotropy spectrum of the cosmic microwave background. A perturbative scheme for the solution of the Wheeler-DeWitt equation has been found to allow for enhancement of power at large scales, whereas the alternative predicts a suppression of power at large scales. Both effects are corrections which, although conceptually interesting, turn out to be too small to be detected. Another scheme relies upon a Born-Oppenheimer analysis: by using a perturbative approach to the nonlinear ordinary differential equation obeyed by the two-point function for scalar fluctuations, a new family of power spectra has been obtained and studied by the authors.

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Is there a quantum gravity effect on the CMB power spectrum?G. Esposito

\bodymatter

1 Introduction

Since the time of its discovery [1], the Cosmic Microwave Background (hereafter CMB) radiation has provided a novel perspective on theoretical and observational cosmology, and recent theoretical developments deal with a careful evaluation of the CMB power spectrum. In particular, the original idea in Ref. \refciteKief12 was to solve via a JWKB method the Wheeler-DeWitt equation in the minisuperspace for a spatially flat FRW universe coupled to a scalar field, and compute the resulting power spectrum. The authors of Ref. \refciteKief12 found a suppressed CMB power spectrum at large scales. However, in Ref. \refciteBini13, the opposite result was obtained. Both papers agreed that the effect was too small to be detected.

Meanwhile, the work by Refs. \refciteKam13,Kam14, relying upon Refs. \refciteBV,Bertoni, developed a Born-Oppenheimer (BO) approach to quantum cosmology that is manifestly unitary. Within this framework, the work in Ref. \refciteBE14 obtained new formulas for the power spectrum, which are assessed hereafter.

2 Nonlinear differential equation obtained from the Born-Oppenheimer method

The analysis is here restricted to minisuperspace for a spatially flat FRW universe coupled to a massive scalar field. By means of a brilliant analysis, the authors of Ref. [4] proved that the 2-point function ( being conformal time) describing the spectrum of scalar fluctuations obeys the equation

(1)

where pertains to the vacuum state that reduces to the Bunch-Davies vacuum [9] in the short wavelength regime, and is found to be

(2)

3 Solutions of the nonlinear differential equation

We now define the variables , and look for solutions in the form

(3)

By defining , the equation for reduces to [8]

(4)

Various particular cases can be solved, e.g.

(5)
(6)

where ; there exists also a polynomial solution for both and , i.e.

(7)

If the ratio is much smaller than , the resulting perturbation can be thrusted, and the very small values of allow for polynomials of large degree.

4 The power spectrum

The basic formula for the power spectrum is very simple, i.e.

(8)

In the three cases studied before, it yields

(9)
(10)

the third case occurring when a second degree polynomial for both and leads to

(11)

The constants can be adjusted to fit the data, but the data are beyond the sensitivity of existing devices (see, however, comments in Sect. 6). The statistical uncertainty in the data is much larger than the correction in Ref. \refciteBini13.

5 Higher degree polynomials; powers of and

In Ref. \refciteBE14, we have obtained a sixth-degree polynomial for and , with power spectrum

(12)

One can also consider solutions which involve both negative and positive powers of . Interestingly, a particular solution exists for which

(13)
(14)

The resulting power spectrum is

(15)

which has therefore an enhancement factor equal to , whose average is equal to , if defined as a principal-value integral [8].

6 Results and new perspectives

(i) Our formulas for the power spectrum reduce to existing ones in particular cases, but have better potentialities, because the lower and upper limit of summation for and are arbitrary. (ii) The work in Ref. \refciteKam14 has evaluated the spectra of scalar and tensor perturbations to first order in the slow-roll approximation, which provides new quantum gravity effects with respect to pure de Sitter. (iii) The work in Ref. \refciteKam15 has found that the effect of quantum gravitational corrections compared to the standard cases leads to a better fit with the data. The possibility of understanding the loss in power as an effect of quantum gravity on standard slow-roll inflation is an entirely new perspective, and the results by these authors suggest looking for quantum gravity effects at much smaller scales as well.

Acknowledgments

G. Esposito is grateful to Dipartimento di Fisica of Federico II University, Naples, for hospitality and support. The authors have enjoyed previous collaboration with C. Kiefer, M. Krämer and F. Pessina on related topics, and thank A. Yu. Kamenshchik for correspondence.

References

  1. A. A. Penzias and R. W. Wilson, Astrophys. J. 142, 419 (1965).
  2. C. Kiefer and M. Krämer, Phys. Rev. Lett. 108, 021301 (2012).
  3. D. Bini, G. Esposito, C. Kiefer, M. Krämer, and F. Pessina, Phys. Rev. D87, 104008 (2013).
  4. A. Yu. Kamenshchik, A. Tronconi, and G. Venturi, Phys. Lett. B726, 518 (2013).
  5. A. Yu. Kamenshchik, A. Tronconi, and G. Venturi, Phys. Lett. B734, 72 (2014).
  6. R. Brout and G. Venturi, Phys. Rev. D39, 2436 (1989).
  7. C. Bertoni, F. Finelli, and G. Venturi, Class. Quantum Grav. 13, 2375 (1996).
  8. D. Bini and G. Esposito, Phys. Rev. D89, 084032 (2014).
  9. T. S. Bunch and P. C. W. Davies, Proc. R. Soc. A360, 117 (1978).
  10. A. Yu. Kamenshchik, A. Tronconi, and G. Venturi, JCAP 04, 046 (2015).
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